L. Spinoglio 1, T. Giannini 1, P. Saraceno 1, A. Di Giorgio 1, B. Nisini 1, E. Caux 2, C. Ceccarelli 3, D. Lorenzetti 4, F. Palla 5, H. Smith 6, & G. White 7.
1 Istituto di Fisica dello Spazio Interplanetario - CNR - Roma, Italy
2 CESR, BP4346, F-31028 Toulouse Cedex 04, France
3 Observatoire de Grenoble, BP 53 F-38041, Grenoble, France
4 Osservatorio di Roma, Monteporzio, Italy
5 Osservatorio Astrofisico di Arcetri, I-50125 Firenze, Italy
6 Harvard Smithsonian Center for Astrophysics, MA 02138 Cambridge
7 Queen Mary & Westfield College, London, UK
With the LWS spectrometer on-board the Infrared Space
Observatory (ISO), we have detected toward T Tauri
strong emission from high-J (J>14) CO, H2O and OH transitions
over the wavelength range from 40 to 190 
.
In addition, the LWS spectrum also shows the [OI]63 and 145
and [CII]158
atomic lines.
All the molecular emission can be explained by a single region at
T
300-900 K and n
105-6cm-3,
with a diameter of about 2-3 arcsec, corresponding to 300-400 AU (at the
distance of 140 pc).
We derive a H2O/H
1.5
implying a H2O enhancement
by more than 100 with respect to the ambient gas abundance.
Similarly, from the OH emission lines, we derive an OH/H2 abundance
2.7
,
i.e. twice that of water.
The estimated relatively high density and compactness of the observed emission may suggest that it is originated from the shocks taking place at the base of the molecular outflow emission, in the region where the action of the stellar winds originating from the two stars of the binary system is important.